workshop on iter simulation, beijing, 2006 kuafu team various insitituions c.y. tu, s.y. fu...
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Workshop on ITER Simulation, Beijing, 2006
KuaFu TeamVarious InsitituionsC.Y. Tu, S.Y. Fu
Institute of Space Physics and Applied TechnologySchool of Earth and Space Sciences
Peking University
KuaFu MissionSolar Storm, Aurora and Space Weather Explorer
Workshop on ITER Simulation, Beijing, 2006
Milestones of KuaFu
Jan. 2003---- First proposed by Prof. Chuanyi TuSep. 2003---- Mission is named “KuaFu”……… Presented in many conferences and meetingsSep. 2004---- Supported by CNSF for concept studyDec. 2004---- First group meeting, Frankfurt, GermanyDec. 2004---- Listed in the ILWS-missionsMay 2005---- First international workshop on KuaFu, Beijing.Sep. 2005---- Selected as the potential space mission by CNSA.Jan. 2006---- First science working group meeting in MPS, Lindau, Germany
Workshop on ITER Simulation, Beijing, 2006
General Concept Developing Group
Chuan-Yi Tu Peking University, Beijing, ChinaYong-Wei Zhang DFH Satellite Co. LTD, Beijing, China Jing-Song Wang Peking University, Beijing, China
( China Meteorological Administration)Li-Dong Xia U. Science and Technology of China, Hefei, China
Rainer Schwenn MPS, Lindau, GermanyEric Donovan University of Calgary, Calgary, CanadaEckart Marsch MPS, Lindau, Germany
Zuo Xiao Peking University, Beijing, China Feng-Si Wei Chinese Academy of Sciences, Beijing, China
Workshop on ITER Simulation, Beijing, 2006
Sun-Earth System Exploration
1. The first step is to find the composition of the Sun-Earth system.
Photosphere, corona, solar wind, magnetic cloud, bow shock, magnetopause, plasma sheet, etc. This cartography is largely done.
2. The second step is to observe the correlations and interactions between two phenomena,
between CME and Flare, magnetic cloud and sub-storm, et al.
3. The third step is to explore the complex global behavior. The space storms, such as CMEs and sub-storm and magnetic storm
s are all multiscale phenomena, i.e., interactions occur simultaneously on several distinct scales.
KuaFu Mission concentrates on exploring the complex global behavior
of the Sun- Earth system
Workshop on ITER Simulation, Beijing, 2006
Day of Year, Start time 12:00UT,on July15,2000
‘Bastille Day’ event in the year of 2000
Chain of solar terrestrial disturbance
POLAR: New Views of the
Aurora
Workshop on ITER Simulation, Beijing, 2006
dimming
blast waveflare
eruption
SOHO/EIT
Possible Precursors of CME
What are the real prosses between these precursors and CMEs?
How does CMEs propergate in the interplanetary space?
What is the geo-effect of CMEs? Can we forcast the space weather?
Workshop on ITER Simulation, Beijing, 2006
To observe continually the complete chain of actions/reactions from the solar atmosphere to geo-space:Solar Source of the disturbances Solar flares, CMEs, Energetic particles Transportation of the disturbances interplanetary clouds, radio waves, shock waves, solar energetic particles Geo-effectiveness aurora activities, sub-storms, magnetic storms,
Space Weather Science Objectives
Workshop on ITER Simulation, Beijing, 2006
Solar Science Objectives
•How is the mass supplied to CMEs?•How is the mass supplied to the solar wind?•How is the mass supplied from the cromosphere to the corona?
•What are the precursors of CMEs?•How is the relation between flares and CMEs?•How are the CMEs accelerated? •How the mass losses from the corona?
Workshop on ITER Simulation, Beijing, 2006
1. How does the central plasma sheet (CPS) feeds particles into the ring current? What is the role of sub-storms in storms?
2. Pole-ward boundary intensifications (PBIs) simultaneously in the conjugate hemispheres will give information on time and location of reconnection and also the rates and the associated plasma flows.
3. The energy flux of electrons and protons can be obtained. The source/sink monitoring by KuaFu allows quantitative assessment of geo-effectiveness that is otherwise impossible.
4. KuaFu B integrated imaging provides a natural way to test our modeling capabilities in geo-space science.
Geo-space Science Objectives
Workshop on ITER Simulation, Beijing, 2006
Imaging the Source region• Solar EUV emission (195A)• Lyman-alpha Disc imager up to 1.1Rs Tracing the CMEs, etc• Lyman-alpha coronagraph 1.1-2.5 Rs• White light coronagraph 2.5-15 Rs• Radio wave measurement (1Rs-L1) In situ• Local plasma and magnetic field (L1)• High energy particles (L1)
KuaFu-A
Workshop on ITER Simulation, Beijing, 2006
Lyman-alpha coronagraph 1.1-2.5 Rs
Lyman-alpha Disc imager up to 1.1Rs
White light coronagraph 2.5-15 Rs
A LASCO C2 "running difference" image showing a "halo" CME blast beginning its journey towards Earth on 7 April 1997
Workshop on ITER Simulation, Beijing, 2006
Imager1. UV imagers (primarily electron aurora) 24 hours.2. Lyman-alpha imaging spectrograph (24 hours)3. Wide FOV perigee imager for conjugate (perigee) imaging.4. Energetic Neutral Atoms (ENA) imager for ring current observations (24 hours).
In situ 5. Fluxgate Magnetometer ( FGM).6. High energy proton observations (HEPS) 7. Plasma Spectrometer (FPI/IMS)
KuaFu-B
Workshop on ITER Simulation, Beijing, 2006
The complete chain of disturbancefrom the solar atmosphere to the geo-space
Lyman αCoronagraph
White Light Coronagraph
Radio Wave measurement
MF, PlasmaHigh energy particle
Auroral image24 hours/day
Ionosphere
Auroral image conjugate
Ground base Auroral measurement
Disk Lyman α chromosphere
Disk 195Ǻ corona
PhenomenaFilament eruptions
Flares CMEs Shock wavesM. Clouds
SubstormPBS
Storm
New science objectives:Precursor of Eruption
Origin and developmentof flares and CMEs
3D geometry expansionof CMEs (synthesized with Solar Orbitor and Sentinels)
Tail Reconnection
Energy sink during storm and substorm
Energetic Neutron Atom(ENA) 24 hours
Kuafu AKuafu B1Kuafu B2
15 Rs2.5 Rs
Workshop on ITER Simulation, Beijing, 2006
Review of the Assessment Report
The overall mission report achieved a simple average score of 3.3 out of a maximum of 4.0. (4 – excellent, 3 – very good)--- William Liu(Chair ILWS Steering Committee)
Workshop on ITER Simulation, Beijing, 2006
Endorsement for KuaFu Payload
"The SSWG (Solar System Working Group, ESA) found the described mission concept is good and noted a widespread interest within the relevant scientific community in Europe. The SSWG therefore endorses payload participation by national agencies in this mission …
------ Prof. Dr. Robert F. Wimmer-Schweingruber, University of Kiel
Workshop on ITER Simulation, Beijing, 2006
Payload of KuaFu-A (updated in Jan. 2006)
Instrument Mass(kg)
PIs
EUV/FUV disk imager (EDI),including a Lyman-alpha disk imager Polarimeter
252
P. Rochus (Belgium)U. Schühle ( Germany )
Coronal Dynamics Imager (CDI),including a Lyman-alpha coronagraph
45 P. Lamy ( France )
Radio Burst Instrument (RBI) 11 J.-L. Bougeret ( France)
Solar Wind Instrument Package (SWIP) 67
R. Schwenn K.-H. Glassmeier(Germany)
C.M. Carr ( UK)
Solar Energetic Particle Sensor(SEPS) 6.5 R. Wimmer-Schweingruber ( Germany )
S.-J. Wang (China )Hard X-Ray and Gamma-Ray
Spectrometer(HXGR) 4.5 G.-W. Qun ( China )
Solar Irradiance Measurement (SIM) 13 D.-R. Lü ( China ) W. Schmutz ( Swithzland )
Multi-Order Solar EUV Spectrograph (MOSES) 10 L. Harra ( UK ) Total 130
Workshop on ITER Simulation, Beijing, 2006
L.-D. Xia University of Science and Technology of China (Convener)R. Schwenn Max Planck Institute for Solar System Research, GermanyE. Marsch Max Planck Institute for Solar System Research, GermanyP. Rochus University of Liege, BelgiumP. Lamy Laboratoire d'Astrphysique de Marseille, FranceJ.-L. Bougeret Centre National de la Recherche Scientifique, FranceU. Schühle Max Planck Institute for Solar System Research, GermanyR. Wimmer-Schweingruber Kiel University, GermanyK.-H. Glassmeier Braunschweig University, GermanyC. M. Carr Imperial College London, United KindomW.-Q. Gan Chinese Academy of Sciences, ChinaJ. Chang Chinese Academy of Sciences, ChinaS.-J.Wang Chinese Academy of Sciences, China
KuaFu-A Group
Workshop on ITER Simulation, Beijing, 2006
Instrument Mass(kg) Power(W) Proposal PI
Far Ultraviolet Auroral Monitoring Camera (UVAMC)
21 11Canada
E. DonovanT. S. Trondsen
FUV Imaging Spectrometer (FUVSI) 20 4.4 Belgium C. Jamar
Wide Field Auroral Imager (WFAI) 1.5 10 UK M. Lester
Fluxgate Magnetometer (FGM) 3 4.25 Austria T.-L. Zhang
High Energy Charged Particle Experiment(HECPE)
3 4China H. F. Chen
Medium-Energy Particle Imager (IEPS)
5.6 4.5UK/China
M. Dunlop/H.F. Chen
Neutral Atom Imager on KuaFu (NAIK)
6 4 Ireland/China
S. McKenna-Lawlor
Fast Plasma Pitch angle Anylazer (FPI)
6 10 UK A. Fazakerley
Ion Mass Spectrometer(IMS) 3.5 2.5 France H. Reme
Tri-Band Beacon (TBB) 3.5 1 China J. Wu
Total 73 ~56
Payload of KuaFu-B (updated in Jan. 2006)
Workshop on ITER Simulation, Beijing, 2006
KuaFu-B Group Jing-Song Wang Peking University, China (Convener)E. Donovan University of Calgary, CanadaTrond S. Trondsen University of Calgary, CanadaM. Lester Leicester University, United KindomT. –L. Zhang Austrian Academy of Sciences, AustriaS. McKenna-Lawlor National University of Ireland, IrelandM. Dunlop Rutherford Appleton Laboratory, United KindomC. Jamar University of Liege, BelgiumS.-Y. Fu Peking University, ChinaH.-F. Chen Peking University, ChinaL. Xie Peking University, ChinaJ. Wu China Research Institute of Radiowave Propagation, ChinaD.-H. Zhang Peking University, China
Workshop on ITER Simulation, Beijing, 2006
Where are we now?
The "comprehensive review" of the KuaFu project supported by CNSA started beginning 2006………… Launch in 2012 ( SolarMax)
Workshop on ITER Simulation, Beijing, 2006
Stamp Published on Sept 25th,1987,by Beijing Stamp Printers.
One day Mr. KuaFu tried to catch up with the sun and to enter into it. As he was terribly thirsty, he went to drink in the Yellow River and the Wei River ,but the water in the two rivers was not enough for him, so he turned northward to the sea. Before he could reach there he died of thirst. And his stick was lost in the wild field and it grew up into a forest (Deng-Lin)."
KuaFu-An ancient Chinese myth
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